论文标题
金属差星形区域麦哲伦桥C中解决的恒星形成C
Resolved star formation in the metal poor star-forming region Magellanic Bridge C
论文作者
论文摘要
Magellanic Bridge C（MB-C）是一种金属贫困（$ \ sim $ 1/5 $ z {\ odot} $）低密度的星形形成区域，位于麦哲伦桥上59 kpc，在与Galaxy不同的条件下提供了恒星形成过程的解决方案。从Atacama大毫米阵列CO（1-0）观测值中，我们检测到与候选年轻恒星对象（YSO），前序列（PMS）恒星（PMS）恒星和丝状结构相关的分子团。 YSO和PMS星形在分子气体中形成，其密度在17-200 $ m _ {\ odot} $ PC $^{ - 2} $之间，并且具有$ \ Lessim $ 0.1-3 Myr。 MB-C中的YSO候选者的消失率低于银河系。否则，我们的结果表明，MB-C中分子团，YSO和PMS星的特性和形态与其银河系相对的同类产品没有专利差异，暂时表明，与MB-C相似的区域中形成的恒星是原子质与分子气的转化。
Magellanic Bridge C (MB-C) is a metal-poor ($\sim$1/5 $Z_{\odot}$) low-density star-forming region located 59 kpc away in the Magellanic Bridge, offering a resolved view of the star formation process in conditions different to the Galaxy. From Atacama Large Millimetre Array CO (1-0) observations, we detect molecular clumps associated to candidate young stellar objects (YSOs), pre-main sequence (PMS) stars, and filamentary structure identified in far-infrared imaging. YSOs and PMS stars form in molecular gas having densities between 17-200 $M_{\odot}$ pc$^{-2}$, and have ages between $\lesssim$0.1-3 Myr. YSO candidates in MB-C have lower extinction than their Galactic counterparts. Otherwise, our results suggest that the properties and morphologies of molecular clumps, YSOs, and PMS stars in MB-C present no patent differences with respect to their Galactic counterparts, tentatively alluding that the bottleneck to forming stars in regions similar to MB-C is the conversion of atomic gas to molecular.
